An assessment of the rotation rates of the host stars of extrasolar planets

The rotation periods of the host stars of extrasolar planets have been asse ssed against those of the Mount Wilson stars, open cluster stars, and evolu tionary stellar models that include rotation. They appear to be normal, mod ulo certain inconsistencies in various necessary inputs. Selection of candi date planet hosts for radial velocity surveys by low rotation or activity h as resulted in a planet host sample skewed toward older stars. Thus, cross- comparisons must be age-dependent. However, self-consistent ages are diffic ult to obtain, and activity ages show signs of systematic errors. There are indications that activity ages ought to be increased for subsolar mass sta rs and decreased for supersolar mass stars. Age uncertainties and a scarcit y of measured rotation periods for planet host stars inflate the dispersion in older stars relative to those in open clusters. The presently available rotational models display inadequacies, most notably in producing fast eno ugh early-type stars. The fact that only one planet host star, tau Boo, str ongly suggests tidal spin-up, while on the order of 10 systems suggest orbi tal circularization is explicable in terms of the differing timescales for these two phenomena. The rotational normalcy of the planet host stars and o ther considerations suggest that they are not especially different from oth er main-sequence stars and that circumstellar matter and/or planets are pro bably ubiquitous, at least among sufficiently metal-rich solar-type stars.